Stijn Wuyts (MPE) Natascha Frster Schreiber (MPE) Benjamin Magnelli - - PowerPoint PPT Presentation

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Stijn Wuyts (MPE) Natascha Frster Schreiber (MPE) Benjamin Magnelli - - PowerPoint PPT Presentation

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A RESOLVED VIEW ON STELLAR POPULATIONS AT COSMIC NOON Stijn Wuyts (MPE) Natascha Frster Schreiber (MPE) Benjamin Magnelli (MPE) Raanan Nordon (MPE) Reinhard Genzel (MPE) Stefano Berta (MPE) Arjen van der Wel (MPIA) Herve Aussel

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SLIDE 1

A RESOLVED VIEW ON STELLAR POPULATIONS AT COSMIC NOON

Stijn Wuyts (MPE)

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SLIDE 2

CANDELS & PEP

Natascha Förster Schreiber (MPE) Reinhard Genzel (MPE) Arjen van der Wel (MPIA) Dieter Lutz (MPE) Yicheng Guo (UMass)

Guillermo Barro (UCSC) Eric Bell (UMichigan) Avishai Dekel (Hebrew University) Sandra Faber (UCSC) Henry Ferguson (STScI) Mauro Giavalisco (UMass) Norman Grogin (STScI) Nimish Hathi (Carnegie) Kuang-Han Huang (Johns Hopkins) Dale Kocevski (UCSC) Anton Koekemoer (STScI) David Koo (UCSC) Benjamin Magnelli (MPE) Raanan Nordon (MPE) Stefano Berta (MPE) Herve Aussel (CEA-Saclay) Emeric Le Floc’h (CEA-Saclay) Javier Gracia-Carpio (MPE) Jennifer Lotz (STScI) Elizabeth McGrath (UCSC) Jeffrey Newman (UPittsburgh) David Rosario (MPE) Amelie Saintonge (MPE) Linda Tacconi (MPE) Benjamin Weiner (UArizona) Antonio Cava (Madrid) Paola Popesso (MPE) Francesca Pozzi (Bologna) Laurie Riguccini (Bologna) Giulia Rodighiero (Padova)

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SLIDE 3

Galaxy properties across the SFR-Mass diagram:

  • normal SFing galaxies
  • high-SFR outliers
  • quenched galaxies

THE RELATION BETWEEN STRUCTURE AND STELLAR POPULATIONS: GLOBALLY & LOCALLY

Mass SFR

Light ≠ Mass Smoother stellar mass maps Short-lived SFing clumps

Wuyts et al. 2012, ApJ, 753, 114 Wuyts et al. 2011, ApJ, 742, 96

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SLIDE 4

Departure from main sequence goes hand in hand with morphological transition

see also Kauffmann et al. 2003; Brinchmann et al. 2004; Schiminovich et al. 2007; Wake et al. 2012 @ z ~ 0.1 Toft et al. 2009; Williams et al. 2009; Szomoru et al. 2011; Bell et al. 2011; Elbaz et al. 2011 @ intermediate & high z

Wuyts et al. 2011b

median size

Disks Spheroids

median nSersic

Main sequence galaxies are the largest at a given mass

0.02 < z < 0.20 0.5 < z < 1.5 1.5 < z < 2.5 0.02 < z < 0.20 0.5 < z < 1.5 1.5 < z < 2.5

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SLIDE 5

median IR/UV median ΣSFR

Obscuration increases along MS, and at a given mass across MS

see also Kauffmann et al. 2003; Brinchmann et al. 2004; Schiminovich et al. 2007; Wake et al. 2012 @ z ~ 0.1 Toft et al. 2009; Williams et al. 2009; Elbaz et al. 2011; Bell et al. 2012; Whitaker et al. 2012 @ intermediate & high z

Wuyts et al. 2011b

High-SFR outliers not just upscaled MS galaxies; more SFR per unit area

→ intenser radiation field, higher ionization parameter, ...

0.02 < z < 0.20 0.5 < z < 1.5 1.5 < z < 2.5 0.02 < z < 0.20 0.5 < z < 1.5 1.5 < z < 2.5

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SLIDE 6

MORE GALAXY PROPERTIES VARYING RELATIVE TO THE MAIN SEQUENCE OF STAR FORMATION

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SLIDE 7

MORE GALAXY PROPERTIES VARYING RELATIVE TO THE MAIN SEQUENCE OF STAR FORMATION

Dust conditions: PAH strength (L8μm/LIR) Elbaz et al. 2011; Nordon et al. 2012 Dust temperature Magnelli et al. 2012b

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SLIDE 8

MORE GALAXY PROPERTIES VARYING RELATIVE TO THE MAIN SEQUENCE OF STAR FORMATION

Dust conditions: PAH strength (L8μm/LIR) Elbaz et al. 2011; Nordon et al. 2012 Dust temperature Magnelli et al. 2012b ISM conditions: [CII]/LIR Gracia-Carpio et al. 2010 αCO Magnelli et al. 2012a

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SLIDE 9

MORE GALAXY PROPERTIES VARYING RELATIVE TO THE MAIN SEQUENCE OF STAR FORMATION

Dust conditions: PAH strength (L8μm/LIR) Elbaz et al. 2011; Nordon et al. 2012 Dust temperature Magnelli et al. 2012b ISM conditions: [CII]/LIR Gracia-Carpio et al. 2010 αCO Magnelli et al. 2012a Star formation law / tdepletion Daddi et al. 2010; Genzel et al. 2010;

Saintonge et al. 2012; Magnelli et al. 2012b; Martig et al. 2009

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SLIDE 10

MORE GALAXY PROPERTIES VARYING RELATIVE TO THE MAIN SEQUENCE OF STAR FORMATION

Dust conditions: PAH strength (L8μm/LIR) Elbaz et al. 2011; Nordon et al. 2012 Dust temperature Magnelli et al. 2012b ISM conditions: [CII]/LIR Gracia-Carpio et al. 2010 αCO Magnelli et al. 2012a Star formation law / tdepletion Daddi et al. 2010; Genzel et al. 2010;

Saintonge et al. 2012; Magnelli et al. 2012b; Martig et al. 2009

Visual classifications of (ir)regular morph Kartaltepe et al. 2011

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SLIDE 11

Mass SFR

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SLIDE 12

Mass SFR

log(M) > 10 & log(SFR/M) > log(1/tH) 323 SFGs @ 0.5 < z < 1.5 326 SFGs @ 1.5 < z < 2.5

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SLIDE 13

ERS + CANDELS-Deep in GOODS-S Resolved SED modeling accounting for integrated photometric constraints UBVizYJHKs[3.6][4.5][5.8][8.0]

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SLIDE 14
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SLIDE 15
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SLIDE 16

GALAXY STRUCTURE IN LIGHT AND MASS

Wuyts et al. 2012

Star-forming galaxies, at low and high z, are smaller and more concentrated in mass than in light.

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SLIDE 17

GALAXY STRUCTURE IN LIGHT AND MASS

Wuyts et al. 2012

Star-forming galaxies, at low and high z, are more concentrated and smoother in mass than in light.

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SLIDE 18

z ~ 1 z ~ 2 Color-coding: (U-V)rest

ΣSFR Σstellar mass

Wuyts et al. 2012 (see also Förster Schreiber et al. 2011; Guo et al. 2011)

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SLIDE 19

CONTRIBUTION OF CLUMPS TO THE TOTAL MASS, SFR, AND LUMINOSITY IN HIGH-REDSHIFT STAR-FORMING GALAXIES

Off-center ‘clumps’ contribute up to ~20% of the total SFR in distant SFGs, but only 2-7% to the integrated stellar mass. Fraction of SFGs that are ‘clumpy’ is a decreasing function of wavelength.

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SLIDE 20

z ~ 1 z ~ 2 Color-coding: (U-V)rest

AV

Wuyts et al. 2012 (see also Förster Schreiber et al. 2011; Guo et al. 2011)

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SLIDE 21

AV

Wuyts et al. 2012

RADIAL EXTINCTION GRADIENTS: BX610 @ Z=2.2 AS CASE EXAMPLE

NMFS et al. (2006/20009/2011a,b); Tacconi et al. (2010; in prep); Genzel et al. (2008/2011b)

Co-added profile Case example

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SLIDE 22

z ~ 1 z ~ 2 Color-coding: (U-V)rest

AV Age

Typical clump age ~ 130 Myr Efficient clump disruption by strong feedback Efficient inward clump migration

Wuyts et al. 2012 (see also Förster Schreiber et al. 2011; Guo et al. 2011)

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SLIDE 23

Guo et al. 2011 Förster Schreiber et al. 2011

Re

RADIAL TRENDS IN CLUMP EVOLUTIONARY STAGE

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SLIDE 24

SIMULATIONS OF CLUMPY DISKS

Ceverino et al. 2010, 2012

  • Typical ages of clumps

100 - 200 Myr, consistent with Wuyts et al. 2012

  • 36-76% more stars in

bulge than in disk component

  • fgas, simulated ~ 0.04 - 0.18

↔ observed fgas ~ 0.45 by Tacconi et al. 2010

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SLIDE 25

SIMULATIONS OF CLUMPY DISKS

Genel et al. 2012 Clump lifetimes 10 - 100 Myr Typical fgas ~ 0.43

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SLIDE 26

Hopkins et al. 2011

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SLIDE 27

STRONG OUTFLOWS FROM INDIVIDUAL SF-ING CLUMPS

Newman et al. 2012

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SLIDE 28

Mass SFR

WFC3 @z=2 WFC3 @z=2

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SLIDE 29

WFC3 @z=2 WFC3 @z=2

Redder, dustier &

  • lder centers

Smaller, smoother & more concentrated mass profiles

Lack of off-center red clumps suggests short lifetimes (e.g. disruption by SF feedback, see Genzel et al. 2011; Newman et al. 2012) or inward migration before they age Red centers, green disks + blue SFing clumps superposed consistent with inside-out disk growth + short-term spatial fluctuations of the SFH which is uniform over longer timescales Lack of off-center red clumps suggests short lifetimes (e.g. disruption by SF feedback, see Genzel et al. 2011; Newman et al. 2012) or inward migration before they age Red centers, green disks + blue SFing clumps superposed consistent with inside-out disk growth + short-term spatial fluctuations of the SFH which is uniform over longer timescales